Spectral Line Variability in Be and Bn Stars

热的、快速旋转的“B”型恒星的光谱吸收线显示出随着时间在谱线上移动的“凸起”。虽然这些隆起最初被认为是以一种可预测的方式周期性地移动，导致了一种解释，即行波（非径向脉动）是罪魁祸首，但新的数据表明，这些隆起经常被遗漏。为了判断这种明显的不可预测性是由不同脉动模式的“跳动”还是由非周期现象引起的，需要长串的光谱数据。在过去，由于国家设施的实际安排和分配问题，长期的“运动”很难进行。1992年初，乔治亚州立大学将投入使用它的新光谱“多望远镜望远镜”。该设施将有一个大的有效光收集功率和一个电荷耦合器件探测器，并将允许PI获得大量数据，以检查快速旋转的B星的“侧面碰撞”现象的频率，并确定其周期性。PI还相信，收集到的大型数据库将使他能够确定非径向脉动是否导致了神秘的快速旋转的“Be”恒星群的偶发性质量损失。

The spectral absorption lines of hot, rapidly rotating "B" type stars show traveling "bumps" which travel across the lines with time. Although these bumps were first thought to move periodically in a predictable way, leading to an interpretation that traveling waves (nonradial pulsations) were responsible, new data indicate that the bumps are often missing. In order to judge whether this apparent unpredictability is caused by the "beating" of different pulsation modes or by an aperiodic phenomenon, long strings of spectroscopic data are needed. In the past long "campaigns" have been difficult to undertake because of practical scheduling and allocation problems at national facilities. In early 1992 Georgia State will put into operation its new spectroscopic "Multi- Telescope Telescope. This facility will have a large effective light gathering power and a Charged-Couple Device detector and will permit the PI to obtain large amounts of data to examine the frequency of the "profile bump" phenomenon in rapidly rotating B stars and to ascertain its periodic nature. The PI also believes that the large database assembled will enable him to determine whether nonradial pulsations are responsible for episodic mass loss in the enigmatic group of rapidly rotating "Be" stars.